Distribution of Captured Planetesimals in Circumplanetary Gas Disks and Implications for Accretion of Regular Satellites

Suetsugu, Ryo; Ohtsuki, Keiji

doi:10.3847/1538-4357/aa692e

Cited by 36 publications

(23 citation statements)

References 31 publications

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“…Figure 4 shows that the distributions of orbital parameters of the objects at the time of their capture are quite similar in the most favorable scenarios of cases 1 and 2. Similar trends were obtained by Suetsugu & Ohtsuki (2017) although they considered that planetesimals initially populate the close vicinity of Jupiter (i.e., the region inside of Jupiter's gap in our configuration) and no other massive object but Jupiter perturbed their orbits. It should be noted that the distribution of objects in Figure 4 is not representative of the system at a particular time because the planetesimals were not all captured concurrently.…”

Section: Evolution Of Captured Planetesimalssupporting

confidence: 85%

“…It would be surprising were such a reservoir to have existed close to Jupiter and not play any role in the formation of its regular satellites, the origin of whose building blocks remains elusive. Yet, as demonstrated by Suetsugu & Ohtsuki (2017), if the objects of the reservoir were on circular and coplanar orbits, as expected from their formation process, they would have mainly remained out of Jupiter's reach. However, there is now little doubt that Saturn once was orbiting much closer to Jupiter than it is currently (see e.g., Deienno et al 2017, and references therein).…”

Section: Existence Of a Reservoir Of Planetesimals Close To Jupitermentioning

confidence: 91%

“…Another potential mechanism to deliver solid material to the CPD is the capture/ablation of larger planetesimals located in the vicinity of Jupiter due to either collisions in a gas poor environment (Estrada & Mosqueira 2006) or gas drag within a gas rich CPD (Mosqueira et al 2010). The latter process has been numerically investigated by several authors (Fujita et al 2013;Suetsugu et al 2016;Suetsugu & Ohtsuki 2017;D'Angelo & Podolak 2015). However, the existence of planetesimals in the close vicinity of Jupiter is questionable.…”

Section: Capture Of Large Planetesimalsmentioning

confidence: 99%

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Saturn’s Formation and Early Evolution at the Origin of Jupiter’s Massive Moons

Ronnet

Mousis

Vernazza

et al. 2018

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The four massive Galilean satellites are believed to have formed within a circumplanetary disk during the last stages of Jupiter's formation. While the existence of a circum-jovian disk is supported by hydrodynamic simulations, no consensus exists regarding the origin and delivery mechanisms of the building blocks of the forming satellites. The opening of a gap in the circumsolar disk would have efficiently isolated Jupiter from the main sources of solid material. However, a reservoir of planetesimals should have existed at the outer edge of Jupiter's gap, where solids were trapped and accumulated over time. Here we show that the formation of Saturn's core within this reservoir, or its prompt inward migration, allows planetesimals to be redistributed from this reservoir towards Jupiter and the inner Solar System, thereby providing enough material to form the Galilean satellites and to populate the Main Belt with primitive asteroids. We find that the orbit of planetesimals captured within the circumjovian disk are circularized through friction with gas in a compact system comparable to the current radial extent of the Galilean satellites. The decisive role of Saturn in the delivery mechanism has strong implications for the occurrence of massive moons around extrasolar giant planets as they would preferentially form around planets within multiple planet systems.

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Section: Evolution Of Captured Planetesimalssupporting

confidence: 85%

Section: Existence Of a Reservoir Of Planetesimals Close To Jupitermentioning

confidence: 91%

Section: Capture Of Large Planetesimalsmentioning

confidence: 99%

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Saturn’s Formation and Early Evolution at the Origin of Jupiter’s Massive Moons

Ronnet

Mousis

Vernazza

et al. 2018

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“…We aim to find a way to form a system with only one large moon in a CPD. The feasibility of satellitesimal formation has been examined by Shibaike et al (2017) and delivery of solid matereal to a CPD has been discussed by Fujita et al (2012); Tanigawa et al (2014); Suetsugu & Ohtsuki (2017); Ronnet et al (2018). We focus on the later stage of the satellite formation and investigate the orbital evolution of the moons in a dissipating CPD to determine the final appearance of the system.…”

Section: Introductionmentioning

confidence: 99%

Formation of single-moon systems around gas giants

Fujii

Ogihara

2020

A&A

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Context. Several mechanisms have been proposed to explain the formation process of satellite systems, and relatively large moons are thought to be born in circumplanetary disks. Making a single-moon system is known to be more difficult than multiple-moon or moonless systems. Aims. We aim to find a way to form a system with a single large moon, such as Titan around Saturn. We examine the orbital migration of moons, which change their direction and speed depending on the properties of circumplanetary disks. Methods. We modeled dissipating circumplanetary disks with taking the effect of temperature structures into account and calculated the orbital evolution of Titan-mass satellites in the final evolution stage of various circumplanetary disks. We also performed N-body simulations of systems that initially had multiple satellites to see whether single-moon systems remained at the end. Results. The radial slope of the disk-temperature structure characterized by the dust opacity produces a patch of orbits in which the Titan-mass moons cease inward migration and even migrate outward in a certain range of the disk viscosity. The patch assists moons initially located in the outer orbits to remain in the disk, while those in the inner orbits fall onto the planet. Conclusions. We demonstrate for the first time that systems can form that have only one large moon around giant planet. Our N-body simulations suggest satellite formation was not efficient in the outer radii of circumplanetary disks.

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“…Suetsugu et al (2016) and Suetsugu & Ohtsuki (2017) examined the captures and subsequent orbital evolutions of planetesimals. They showed that the capture hypothesis could roughly reproduce the initial radial distribution of planetesimals (i.e.…”

Section: Introductionmentioning

confidence: 99%

Satellitesimal Formation via Collisional Dust Growth in Steady Circumplanetary Disks

Shibaike

Okuzumi

Sasaki

et al. 2017

ApJ

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The icy satellites around Jupiter are considered to have formed in a circumplanetary disk. While previous models focused on the formation of satellites starting from satellitesimals, the question of how satellitesimals form from smaller dust particles has not been addressed so far. In this work, we study the possibility that satellitesimals form in situ in a circumplanetary disk. We calculate the radial distribution of the surface density and representative size of icy dust particles that grow by colliding with each other and drift toward the central planet in a steady circumplanetary disk with a continuous supply of gas and dust from the parent protoplanetary disk. The radial drift barrier is overcome if the ratio of the dust to gas accretion rates onto the circumplanetary disk,Ṁ d /Ṁ g , is high and the strength of turbulence, α, is not too low. The collision velocity is lower than the critical velocity of fragmentation when α is low. Taken together, we find that the conditions for satellitesimal formation via dust coagulation are given byṀ d /Ṁ g ≥ 1 and 10 −4 ≤ α < 10 −2 . The former condition is generally difficult to achieve, suggesting that the in-situ satellitesimal formation via particle sticking is viable only under an extreme condition. We also show that neither satellitesimal formation via the collisional growth of porous aggregates nor via streaming instability is viable as long asṀ d /Ṁ g is low.

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Distribution of Captured Planetesimals in Circumplanetary Gas Disks and Implications for Accretion of Regular Satellites

Cited by 36 publications

References 31 publications

Saturn’s Formation and Early Evolution at the Origin of Jupiter’s Massive Moons

Saturn’s Formation and Early Evolution at the Origin of Jupiter’s Massive Moons

Formation of single-moon systems around gas giants

Satellitesimal Formation via Collisional Dust Growth in Steady Circumplanetary Disks

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